Abstract

The paper presents results of studying the kinematics of the ionized gas in the galaxy of the Large Magellanic Cloud type NGC 7292 obtained with the 2.5-m telescope of the Caucasian Mountain Observatory (CMO SAI MSU) and the 6-m BTA telescope of the Special Astrophysical Observatory (SAO RAS). Analysis of the velocity fields of the ionized and neutral hydrogen showed that the kinematic center of NGC 7292 located at the center of the bar, northwest of the photometric center of the galaxy (the southeastern end of the bar) previously taken as the center of NGC 7292. In addition to the circular rotation of the gas, the radial motions associated with the bar play a significant role in the kinematics of the disk. The observed perturbations of the gaseous-disk kinematics induced by the ongoing star formation do not exceed those caused by the bar. It is possible that part of the non-circular motions (at the southeastern end of the bar which is the brightest H II region) may be related to the effects of the capture of a dwarf companion or a gaseous cloud.

中文翻译：

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麦哲伦型星系 NGC 7292 中的气体运动学

摘要

本文介绍了利用高加索山天文台 (CMO SAI MSU) 的 2.5 米望远镜和特别委员会的 6 米 BTA 望远镜获得的大麦哲伦星云 NGC 7292 星系中电离气体运动学的研究结果。天体物理观测站（SAO RAS）。对电离氢和中性氢速度场的分析表明，NGC 7292的运动中心位于条形中心，位于先前作为NGC中心的星系光度中心（条形东南端）的西北方向7292. 除了气体的圆周旋转之外，与棒相关的径向运动在圆盘的运动学中也起着重要作用。观察到的由正在进行的恒星形成引起的气态盘运动学的扰动不超过由棒引起的扰动。部分非圆形运动（在条带的东南端，即最亮的 H II 区域）可能与捕获矮星伴星或气态云的影响有关。